Dynamical evolution of the Cybele asteroids

@article{Carruba2015DynamicalEO,
  title={Dynamical evolution of the Cybele asteroids},
  author={Valerio Carruba and David Nesvorn'y and Safwan Aljbaae and M. E. Huaman},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2015},
  volume={451},
  pages={244-256}
}
The Cybele region, located between the 2J:-1A and 5J:-3A mean-motion resonances, is adjacent and exterior to the asteroid main belt. An increasing density of three-body resonances makes the region between the Cybele and Hilda populations dynamically unstable, so that the Cybele zone could be considered the last outpost of an extended main belt. The presence of binary asteroids with large primaries and small secondaries suggested that asteroid families should be found in this region, but only… Expand
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References

SHOWING 1-10 OF 32 REFERENCES
The stable archipelago in the region of the Pallas and Hansa dynamical families
Among highly inclined asteroids, the region of the central main belt between the 3J:–1A and 5J:–2A mean-motion resonances has long been known to host the Pallas and Hansa dynamical families. ThisExpand
Constraining the cometary flux through the asteroid belt during the late heavy bombardment
In the Nice model, the late heavy bombardment (LHB) is related to an orbital instability of giant planets which causes a fast dynamical dispersion of a transneptunian cometary disk. We study effectsExpand
The peculiar case of the Agnia asteroid family
The Agnia asteroid family, a cluster of asteroids located near semimajor axis a = 2.79 AU, has experienced significant dynamical evolution over its lifetime. The family, which was likely created byExpand
Orbital evolution of the Gefion and Adeona asteroid families: close encounters with massive asteroids and the Yarkovsky effect
Abstract Asteroid families are groupings of minor planets identified by clustering in their proper orbital elements; these objects have spectral signatures consistent with an origin in the break-upExpand
Dynamical evolution and chronology of the Hygiea asteroid family
The asteroid (10) Hygiea is the fourth largest asteroid of the main belt, by volume and mass, and it is the largest member of its own family. Previous works investigated the long-term effects ofExpand
The (not so) peculiar case of the Padua family
The Agnia asteroid family was recently studied by Vokrouhlicky et al. because of its peculiar and, so far, unique relationship with the z 1 secular resonance. The Agnia family is almost entirelyExpand
Yarkovsky footprints in the Eos family
Abstract The Eos asteroid family is the third most populous, after Themis and Koronis, and one of the largest non-random groups of asteroids in the main belt. It has been known and studied forExpand
Collisionally Born Family About 87 Sylvia
There are currently more than 1000 multi-opposition objects known in the Cybele population, adjacent and exterior to the asteroid main belt, allowing a more detailed analysis than was previouslyExpand
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model
Abstract Asteroid (101955) Bennu, the target of NASA’s OSIRIS-REx sample return mission, is a D ≈ 0.5  km diameter low albedo near-Earth object. It has a spectral signature consistent with primitiveExpand
A Semianalytical Model for the Motion of the Trojan Asteroids: Proper Elements and Families
In this paper we develop a semianalytical model to describe the long-term motion of Trojan asteroids located in tadpole orbits around the L4 and L5 jovian Lagrangian points. The dynamical model isExpand
...
1
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4
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